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Development of 15 micron cutoff wave...

Cabrera, Mario.

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Development of 15 micron cutoff wavelength HgCdTe detector arrays for astronomy

紀錄類型:	書目-電子資源 : Monograph/item
正題名/作者:	Development of 15 micron cutoff wavelength HgCdTe detector arrays for astronomy/ by Mario Cabrera.
作者:	Cabrera, Mario.
出版者:	Cham :Springer International Publishing : : 2020.,
面頁冊數:	xvii, 121 p. :ill., digital ;24 cm.
內容註:	Chapter1: Introduction -- Chapter2: Test and Data Acquisition Setup -- Chapter3: Dark Current Theory -- Chapter4: Array Characterization -- Chapter5: Phase I Results: 13 m Cuto Wavelength Devices -- Chapter6: Phase II Results: 15 m Cuto Wavelength Devices -- Chapter7: Conclusions and Future Work.
Contained By:	Springer Nature eBook
標題:	Infrared array detectors. -
電子資源:	https://doi.org/10.1007/978-3-030-54241-2
ISBN:	9783030542412

Development of 15 micron cutoff wavelength HgCdTe detector arrays for astronomy
Cabrera, Mario.

Development of 15 micron cutoff wavelength HgCdTe detector arrays for astronomy[electronic resource] /by Mario Cabrera. - Cham :Springer International Publishing :2020. - xvii, 121 p. :ill., digital ;24 cm. - Springer theses,2190-5053. - Springer theses..

Chapter1: Introduction -- Chapter2: Test and Data Acquisition Setup -- Chapter3: Dark Current Theory -- Chapter4: Array Characterization -- Chapter5: Phase I Results: 13 m Cuto Wavelength Devices -- Chapter6: Phase II Results: 15 m Cuto Wavelength Devices -- Chapter7: Conclusions and Future Work.

This thesis describes advances in the understanding of HgCdTe detectors. While long wave (15 um) infrared detectors HgCdTe detectors have been developed for military use under high background irradiance, these arrays had not previously been developed for astronomical use where the background irradiance is a billion times smaller. The main pitfall in developing such arrays for astronomy is the pixel dark current which plagues long wave HgCdTe. The author details work on the success of shorter wavelength development at Teledyne Imaging Sensors, carefully modeling the dark current-reverse bias voltage curves of their 10 um devices at a temperature of 30K, as well as the dark current-temperature curves at several reverse biases, including 250 mV. By projecting first to 13 and then 15 um HgCdTe growth, values of fundamental properties of the material that would minimize tunneling dark currents were determined through careful modeling of the dark current-reverse bias voltage curves, as well as the dark current-temperature curves. This analysis was borne out in the 13 um parts produced by Teledyne, and then further honed to produce the necessary parameters for the 15 um growth. The resulting 13 um arrays are being considered by a number of ground-based astronomy research groups.

ISBN: 9783030542412

Standard No.: 10.1007/978-3-030-54241-2doiSubjects--Topical Terms:

2203775
Infrared array detectors.

LC Class. No.: TA1570

Dewey Class. No.: 621.362

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520 $a This thesis describes advances in the understanding of HgCdTe detectors. While long wave (15 um) infrared detectors HgCdTe detectors have been developed for military use under high background irradiance, these arrays had not previously been developed for astronomical use where the background irradiance is a billion times smaller. The main pitfall in developing such arrays for astronomy is the pixel dark current which plagues long wave HgCdTe. The author details work on the success of shorter wavelength development at Teledyne Imaging Sensors, carefully modeling the dark current-reverse bias voltage curves of their 10 um devices at a temperature of 30K, as well as the dark current-temperature curves at several reverse biases, including 250 mV. By projecting first to 13 and then 15 um HgCdTe growth, values of fundamental properties of the material that would minimize tunneling dark currents were determined through careful modeling of the dark current-reverse bias voltage curves, as well as the dark current-temperature curves. This analysis was borne out in the 13 um parts produced by Teledyne, and then further honed to produce the necessary parameters for the 15 um growth. The resulting 13 um arrays are being considered by a number of ground-based astronomy research groups.
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